Journal Article

Proper motion and apparent contraction in J0650+6001

M. Orienti and D. Dallacasa

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 406, issue 1, pages 529-534
Published in print July 2010 | ISSN: 0035-8711
Published online July 2010 | e-ISSN: 1365-2966 | DOI:
Proper motion and apparent contraction in J0650+6001

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We present a multi-epoch and multifrequency very long baseline interferometry (VLBI) study of the compact radio source J0650+6001. In VLBI images, the source is resolved into three components. The central component shows a flat spectrum, suggesting the presence of the core, while the two outer regions, with a steeper spectral index, display a highly asymmetric flux density. The time baseline of the observations considered to derive the source expansion covers about 15 yr. During this time interval, the distance between the two outer components has increased by 0.28 ± 0.13 mas, that corresponds to an apparent separation velocity of 0.39c± 0.18c and a kinematic age of 360 ± 170 yr. On the other hand, a multi-epoch monitoring of the separation between the central and the southern components points out an apparent contraction of about 0.29 ± 0.02 mas, corresponding to an apparent contraction velocity of 0.37c± 0.02c. Assuming that the radio structure is intrinsically symmetric, the high flux density ratio between the outer components can be explained in terms of Doppler beaming effects where the mildly relativistic jets are separating with an intrinsic velocity of 0.43c± 0.04c at an angle between 12° and 28° to the line of sight. In this context, the apparent contraction may be interpreted as a knot in the jet that is moving towards the southern component with an intrinsic velocity of 0.66c± 0.03c, and its flux density is boosted by a Doppler factor of 2.0.

Keywords: radiation mechanisms: non-thermal; quasars: individual: J0650+6001; radio continuum: general

Journal Article.  3773 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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